TRANSITION TO RIGID ROTATION IN THE RADIATIVE ZONE OF THE SUN - THE EFFECT OF A FOSSIL MAGNETIC-FIELD

An explanation in terms of a fossil magnetic field is offered for a th in layer where a transition from differential to rigid-body rotation o ccurs beneath the convective envelope of the Sun. The spatial distribu tions and ohmic-decay times are calculated for various modes of the fo ssil field. The lifetime of the most slowly decaying mode exceeds the age of the Sun. The magnetic field effectively suppresses the differen tial rotation, A poloidal-field strength of similar to 10(-3) G is eno ugh for helioseismological constraints on the depth of penetration of the differential rotation into the radiative zone to be satisfied.